Eclipsing binary science via the merging of transit and doppler exoplanet survey data - A case study with the marvels pilot project and SuperWASP

Scott W. Fleming, Pierre F.L. Maxted, Leslie Hebb, Keivan G. Stassun, Jian Ge, Phillip A. Cargile, Luan Ghezzi, Nathan M. De Lee, John Wisniewski, Bruce Gary, G. F. Porto De Mello, Leticia Ferreira, Bo Zhao, David R. Anderson, Xiaoke Wan, Coel Hellier, Pengcheng Guo, Richard G. West, Suvrath Mahadevan, Don Pollacco & 11 others Brian Lee, Andrew Collier Cameron, Julian C. Van Eyken, Ian Skillen, Justin R. Crepp, Duy Cuong Nguyen, Stephen R. Kane, Martin Paegert, Luiz Nicolaci Da Costa, Marcio A.G. Maia, Basilio X. Santiago

Research output: Contribution to journalArticle

3 Citations (Scopus)

Abstract

Exoplanet transit and Doppler surveys discover many binary stars during their operation that can be used to conduct a variety of ancillary science. Specifically, eclipsing binary stars can be used to study the stellar mass-radius relationship and to test predictions of theoretical stellar evolution models. By cross-referencing 24 binary stars found in the MARVELS Pilot Project with SuperWASP photometry, we find two new eclipsing binaries, TYC 0272-00458-1 and TYC 1422-01328-1, which we use as case studies to develop a general approach to eclipsing binaries in survey data. TYC 0272-00458-1 is a single-lined spectroscopic binary for which we calculate a mass of the secondary and radii for both components using reasonable constraints on the primary mass through several different techniques. For a primary mass of M 1 = 0.92 0.1 M, we find M 2 = 0.610 0.036 M, R 1 = 0.932 0.076 R, and R 2 = 0.559 0.102 R, and find that both stars have masses and radii consistent with model predictions. TYC 1422-01328-1 is a triple-component system for which we can directly measure the masses and radii of the eclipsing pair. We find that the eclipsing pair consists of an evolved primary star (M 1 = 1.163 0.034 M, R 1 = 2.063 0.058 R) and a G-type dwarf secondary (M 2 = 0.905 0.067 M, R 2 = 0.887 0.037 R). We provide the framework necessary to apply this analysis to much larger data sets.

Original languageEnglish (US)
Article number50
JournalAstronomical Journal
Volume142
Issue number2
DOIs
StatePublished - Aug 1 2011

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extrasolar planets
transit
radii
binary stars
eclipsing binary stars
stars
stellar evolution
predictions
stellar mass
photometry
prediction
pilot project
science

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Fleming, Scott W. ; Maxted, Pierre F.L. ; Hebb, Leslie ; Stassun, Keivan G. ; Ge, Jian ; Cargile, Phillip A. ; Ghezzi, Luan ; De Lee, Nathan M. ; Wisniewski, John ; Gary, Bruce ; Porto De Mello, G. F. ; Ferreira, Leticia ; Zhao, Bo ; Anderson, David R. ; Wan, Xiaoke ; Hellier, Coel ; Guo, Pengcheng ; West, Richard G. ; Mahadevan, Suvrath ; Pollacco, Don ; Lee, Brian ; Collier Cameron, Andrew ; Van Eyken, Julian C. ; Skillen, Ian ; Crepp, Justin R. ; Cuong Nguyen, Duy ; Kane, Stephen R. ; Paegert, Martin ; Nicolaci Da Costa, Luiz ; Maia, Marcio A.G. ; Santiago, Basilio X. / Eclipsing binary science via the merging of transit and doppler exoplanet survey data - A case study with the marvels pilot project and SuperWASP. In: Astronomical Journal. 2011 ; Vol. 142, No. 2.
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abstract = "Exoplanet transit and Doppler surveys discover many binary stars during their operation that can be used to conduct a variety of ancillary science. Specifically, eclipsing binary stars can be used to study the stellar mass-radius relationship and to test predictions of theoretical stellar evolution models. By cross-referencing 24 binary stars found in the MARVELS Pilot Project with SuperWASP photometry, we find two new eclipsing binaries, TYC 0272-00458-1 and TYC 1422-01328-1, which we use as case studies to develop a general approach to eclipsing binaries in survey data. TYC 0272-00458-1 is a single-lined spectroscopic binary for which we calculate a mass of the secondary and radii for both components using reasonable constraints on the primary mass through several different techniques. For a primary mass of M 1 = 0.92 0.1 M, we find M 2 = 0.610 0.036 M, R 1 = 0.932 0.076 R, and R 2 = 0.559 0.102 R, and find that both stars have masses and radii consistent with model predictions. TYC 1422-01328-1 is a triple-component system for which we can directly measure the masses and radii of the eclipsing pair. We find that the eclipsing pair consists of an evolved primary star (M 1 = 1.163 0.034 M, R 1 = 2.063 0.058 R) and a G-type dwarf secondary (M 2 = 0.905 0.067 M, R 2 = 0.887 0.037 R). We provide the framework necessary to apply this analysis to much larger data sets.",
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Fleming, SW, Maxted, PFL, Hebb, L, Stassun, KG, Ge, J, Cargile, PA, Ghezzi, L, De Lee, NM, Wisniewski, J, Gary, B, Porto De Mello, GF, Ferreira, L, Zhao, B, Anderson, DR, Wan, X, Hellier, C, Guo, P, West, RG, Mahadevan, S, Pollacco, D, Lee, B, Collier Cameron, A, Van Eyken, JC, Skillen, I, Crepp, JR, Cuong Nguyen, D, Kane, SR, Paegert, M, Nicolaci Da Costa, L, Maia, MAG & Santiago, BX 2011, 'Eclipsing binary science via the merging of transit and doppler exoplanet survey data - A case study with the marvels pilot project and SuperWASP', Astronomical Journal, vol. 142, no. 2, 50. https://doi.org/10.1088/0004-6256/142/2/50

Eclipsing binary science via the merging of transit and doppler exoplanet survey data - A case study with the marvels pilot project and SuperWASP. / Fleming, Scott W.; Maxted, Pierre F.L.; Hebb, Leslie; Stassun, Keivan G.; Ge, Jian; Cargile, Phillip A.; Ghezzi, Luan; De Lee, Nathan M.; Wisniewski, John; Gary, Bruce; Porto De Mello, G. F.; Ferreira, Leticia; Zhao, Bo; Anderson, David R.; Wan, Xiaoke; Hellier, Coel; Guo, Pengcheng; West, Richard G.; Mahadevan, Suvrath; Pollacco, Don; Lee, Brian; Collier Cameron, Andrew; Van Eyken, Julian C.; Skillen, Ian; Crepp, Justin R.; Cuong Nguyen, Duy; Kane, Stephen R.; Paegert, Martin; Nicolaci Da Costa, Luiz; Maia, Marcio A.G.; Santiago, Basilio X.

In: Astronomical Journal, Vol. 142, No. 2, 50, 01.08.2011.

Research output: Contribution to journalArticle

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T1 - Eclipsing binary science via the merging of transit and doppler exoplanet survey data - A case study with the marvels pilot project and SuperWASP

AU - Fleming, Scott W.

AU - Maxted, Pierre F.L.

AU - Hebb, Leslie

AU - Stassun, Keivan G.

AU - Ge, Jian

AU - Cargile, Phillip A.

AU - Ghezzi, Luan

AU - De Lee, Nathan M.

AU - Wisniewski, John

AU - Gary, Bruce

AU - Porto De Mello, G. F.

AU - Ferreira, Leticia

AU - Zhao, Bo

AU - Anderson, David R.

AU - Wan, Xiaoke

AU - Hellier, Coel

AU - Guo, Pengcheng

AU - West, Richard G.

AU - Mahadevan, Suvrath

AU - Pollacco, Don

AU - Lee, Brian

AU - Collier Cameron, Andrew

AU - Van Eyken, Julian C.

AU - Skillen, Ian

AU - Crepp, Justin R.

AU - Cuong Nguyen, Duy

AU - Kane, Stephen R.

AU - Paegert, Martin

AU - Nicolaci Da Costa, Luiz

AU - Maia, Marcio A.G.

AU - Santiago, Basilio X.

PY - 2011/8/1

Y1 - 2011/8/1

N2 - Exoplanet transit and Doppler surveys discover many binary stars during their operation that can be used to conduct a variety of ancillary science. Specifically, eclipsing binary stars can be used to study the stellar mass-radius relationship and to test predictions of theoretical stellar evolution models. By cross-referencing 24 binary stars found in the MARVELS Pilot Project with SuperWASP photometry, we find two new eclipsing binaries, TYC 0272-00458-1 and TYC 1422-01328-1, which we use as case studies to develop a general approach to eclipsing binaries in survey data. TYC 0272-00458-1 is a single-lined spectroscopic binary for which we calculate a mass of the secondary and radii for both components using reasonable constraints on the primary mass through several different techniques. For a primary mass of M 1 = 0.92 0.1 M, we find M 2 = 0.610 0.036 M, R 1 = 0.932 0.076 R, and R 2 = 0.559 0.102 R, and find that both stars have masses and radii consistent with model predictions. TYC 1422-01328-1 is a triple-component system for which we can directly measure the masses and radii of the eclipsing pair. We find that the eclipsing pair consists of an evolved primary star (M 1 = 1.163 0.034 M, R 1 = 2.063 0.058 R) and a G-type dwarf secondary (M 2 = 0.905 0.067 M, R 2 = 0.887 0.037 R). We provide the framework necessary to apply this analysis to much larger data sets.

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